Gaia16apd - A link between fast and slowly declining type I superluminous supernovae

T. Kangas, N. Blagorodnova, S. Mattila, P. Lundqvist, M. Fraser, U. Burgaz, E. Cappellaro, J. M. Carrasco Martínez, N. Elias-Rosa, L. K. Hardy, J. Harmanen, E. Y. Hsiao, J. Isern, E. Kankare, Z. Kolaczkowski, Martin Bo Nielsen, T. M. Reynolds, L. Rhodes, A. Somero, M. D. StritzingerL. Wyrzykowski

Research output: Contribution to journalArticle

Abstract

We present ultraviolet (UV), optical and infrared photometry and optical spectroscopy of the type Ic superluminous supernova (SLSN) Gaia16apd (=SN 2016eay), covering its evolution from 26 d before the g-band peak to 234.1 d after the peak. Gaia16apd was followed as a part of the NOT Unbiased Transient Survey (NUTS). It is one of the closest SLSNe known (z = 0.102 ± 0.001), with detailed optical and UV observations covering the peak. Gaia16apd is a spectroscopically typical type Ic SLSN, exhibiting the characteristic blue early spectra with O II absorption, and reaches a peak Mg = -21.8 ± 0.1 mag. However, photometrically it exhibits an evolution intermediate between the fast and slowly declining type Ic SLSNe, with an early evolution closer to the fast-declining events. Together with LSQ12dlf, another SLSN with similar properties, it demonstrates a possible continuum between fast and slowly declining events. It is unusually UV-bright even for an SLSN, reaching a non-K-corrected Muvm2 ≃ -23.3 mag, the only other type Ic SLSN with similar UV brightness being SN 2010gx. Assuming that Gaia16apd was powered by magnetar spin-down, we derive a period of P = 1.9 ± 0.2 ms and a magnetic field of B = 1.9 ± 0.2 × 1014 G for the magnetar. The estimated ejecta mass is between 8 and 16 M, and the kinetic energy between 1.3 and 2.5 × 1052 erg, depending on opacity and assuming that the entire ejecta is swept up into a thin shell. Despite the early photometric differences, the spectra at late times are similar to slowly declining type Ic SLSNe, implying that the two subclasses originate from similar progenitors.

Original languageEnglish (US)
Pages (from-to)1246-1258
Number of pages13
JournalMonthly Notices of the Royal Astronomical Society
Volume469
Issue number1
DOIs
StatePublished - Jan 1 2017

Fingerprint

supernovae
ejecta
magnetars
coverings
erg
kinetic energy
infrared photometry
spectroscopy
shell
magnetic field
opacity
photometry
brightness
continuums
magnetic fields

Keywords

  • Stars: magnetars
  • Stars: massive
  • Supernovae: individual (Gaia16apd)

ASJC Scopus subject areas

  • Astronomy and Astrophysics
  • Space and Planetary Science

Cite this

Kangas, T., Blagorodnova, N., Mattila, S., Lundqvist, P., Fraser, M., Burgaz, U., ... Wyrzykowski, L. (2017). Gaia16apd - A link between fast and slowly declining type I superluminous supernovae. Monthly Notices of the Royal Astronomical Society, 469(1), 1246-1258. https://doi.org/10.1093/mnras/stx833

Gaia16apd - A link between fast and slowly declining type I superluminous supernovae. / Kangas, T.; Blagorodnova, N.; Mattila, S.; Lundqvist, P.; Fraser, M.; Burgaz, U.; Cappellaro, E.; Carrasco Martínez, J. M.; Elias-Rosa, N.; Hardy, L. K.; Harmanen, J.; Hsiao, E. Y.; Isern, J.; Kankare, E.; Kolaczkowski, Z.; Nielsen, Martin Bo; Reynolds, T. M.; Rhodes, L.; Somero, A.; Stritzinger, M. D.; Wyrzykowski, L.

In: Monthly Notices of the Royal Astronomical Society, Vol. 469, No. 1, 01.01.2017, p. 1246-1258.

Research output: Contribution to journalArticle

Kangas, T, Blagorodnova, N, Mattila, S, Lundqvist, P, Fraser, M, Burgaz, U, Cappellaro, E, Carrasco Martínez, JM, Elias-Rosa, N, Hardy, LK, Harmanen, J, Hsiao, EY, Isern, J, Kankare, E, Kolaczkowski, Z, Nielsen, MB, Reynolds, TM, Rhodes, L, Somero, A, Stritzinger, MD & Wyrzykowski, L 2017, 'Gaia16apd - A link between fast and slowly declining type I superluminous supernovae', Monthly Notices of the Royal Astronomical Society, vol. 469, no. 1, pp. 1246-1258. https://doi.org/10.1093/mnras/stx833
Kangas, T. ; Blagorodnova, N. ; Mattila, S. ; Lundqvist, P. ; Fraser, M. ; Burgaz, U. ; Cappellaro, E. ; Carrasco Martínez, J. M. ; Elias-Rosa, N. ; Hardy, L. K. ; Harmanen, J. ; Hsiao, E. Y. ; Isern, J. ; Kankare, E. ; Kolaczkowski, Z. ; Nielsen, Martin Bo ; Reynolds, T. M. ; Rhodes, L. ; Somero, A. ; Stritzinger, M. D. ; Wyrzykowski, L. / Gaia16apd - A link between fast and slowly declining type I superluminous supernovae. In: Monthly Notices of the Royal Astronomical Society. 2017 ; Vol. 469, No. 1. pp. 1246-1258.
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AU - Kangas, T.

AU - Blagorodnova, N.

AU - Mattila, S.

AU - Lundqvist, P.

AU - Fraser, M.

AU - Burgaz, U.

AU - Cappellaro, E.

AU - Carrasco Martínez, J. M.

AU - Elias-Rosa, N.

AU - Hardy, L. K.

AU - Harmanen, J.

AU - Hsiao, E. Y.

AU - Isern, J.

AU - Kankare, E.

AU - Kolaczkowski, Z.

AU - Nielsen, Martin Bo

AU - Reynolds, T. M.

AU - Rhodes, L.

AU - Somero, A.

AU - Stritzinger, M. D.

AU - Wyrzykowski, L.

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N2 - We present ultraviolet (UV), optical and infrared photometry and optical spectroscopy of the type Ic superluminous supernova (SLSN) Gaia16apd (=SN 2016eay), covering its evolution from 26 d before the g-band peak to 234.1 d after the peak. Gaia16apd was followed as a part of the NOT Unbiased Transient Survey (NUTS). It is one of the closest SLSNe known (z = 0.102 ± 0.001), with detailed optical and UV observations covering the peak. Gaia16apd is a spectroscopically typical type Ic SLSN, exhibiting the characteristic blue early spectra with O II absorption, and reaches a peak Mg = -21.8 ± 0.1 mag. However, photometrically it exhibits an evolution intermediate between the fast and slowly declining type Ic SLSNe, with an early evolution closer to the fast-declining events. Together with LSQ12dlf, another SLSN with similar properties, it demonstrates a possible continuum between fast and slowly declining events. It is unusually UV-bright even for an SLSN, reaching a non-K-corrected Muvm2 ≃ -23.3 mag, the only other type Ic SLSN with similar UV brightness being SN 2010gx. Assuming that Gaia16apd was powered by magnetar spin-down, we derive a period of P = 1.9 ± 0.2 ms and a magnetic field of B = 1.9 ± 0.2 × 1014 G for the magnetar. The estimated ejecta mass is between 8 and 16 M⊙, and the kinetic energy between 1.3 and 2.5 × 1052 erg, depending on opacity and assuming that the entire ejecta is swept up into a thin shell. Despite the early photometric differences, the spectra at late times are similar to slowly declining type Ic SLSNe, implying that the two subclasses originate from similar progenitors.

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